Coordinated monitoring of the eccentric O-star binary Iota Orionis: optical spectroscopy and photometry

Марченко, С. В.; Rauw, Grégor; Antokhina, É. A.; Antokhin, I. I.; Ballereau, D.; Chauville, J.; Corcoran, M. F.; Costero, R.; Echevarría, J.; Eversberg, Thomas; Gayley, K. G.; Koenigsberger, Gloria; Мирошниченко, А. С.; Moffat, A. F. J.; Morrell, N.; Morrison, N. D.; Mulliss, Christopher L.; Pittard, J. M.; Stevens, I. R.; Vreux, Jean-Marie; Zorec, J.

doi:10.1046/j.1365-8711.2000.03542.x

Cited by 19 publications

(32 citation statements)

References 37 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…At first sight, this is somewhat reminiscent of the case of ι Ori . ASCA observations of ι Ori (O9 III + B1 III, e = 0.764, Marchenko et al 2000) failed to reveal the expected variability between the periastron and apastron phases. However, in the case of HD 93403, we do observe a phase-dependence of the observed X-ray flux.…”

Section: Discussionmentioning

confidence: 95%

Phase-resolved X-ray and optical spectroscopy of the massive binary HD 93403

Rauw

Vreux

Stevens

et al. 2002

A&A

View full text Add to dashboard Cite

Abstract.We report the first results of a campaign aimed at the study of early-type binaries with the XMMNewton observatory. Phase-resolved EPIC spectroscopy of the eccentric binary HD 93403 reveals a clear orbital modulation of the X-ray luminosity as a function of the orbital phase. Below 1.0 keV, the observed X-ray flux is modulated by the opacity of the primary wind. Above 1.0 keV, the observed variation of the X-ray flux is roughly consistent with a 1/r dependence expected for an adiabatic colliding wind interaction. HD 93403 appears less overluminuous in X-rays than previously thought and a significant fraction of the total X-ray emission arises probably within the winds of the individual components of the binary. Optical monitoring of the system reveals strong variability of the He ii λ 4686 and Hα line profiles. The He ii λ 4686 line displays a broad asymmetrical emission component which is found to be significantly stronger between phases 0.80 and 0.15 than around apastron. This suggests that part of the emission arises in the interaction region and most probably in the trailing arm of a shock cone wrapped around the secondary. Some absorption lines of the secondary's spectrum display equivalent width variations reminiscent of the so-called Struve-Sahade effect. The differences in behaviour between individual lines suggest that the temperature may not be the only relevant parameter that controls this effect.

show abstract

Section: Discussionmentioning

confidence: 95%

Phase-resolved X-ray and optical spectroscopy of the massive binary HD 93403

Rauw

Vreux

Stevens

et al. 2002

A&A

View full text Add to dashboard Cite

show abstract

“…These authors also found no evidence of any systematic profile deviations which are associated with non-radial pulsations. The latest optical monitoring (Marchenko et al 2000) again obtained data consistent with a proximity effect.…”

mentioning

confidence: 59%

“…It also emphasizes the poor phase sampling and serves as a useful highlight as to one of the reasons why the latest ASCA data presented in this paper were obtained. In column 3 we list the orbital phase at the time of observation, calculated from the ephemeris HJD periastron 2451 121X658 1 29X133 76E derived from the latest optical monitoring of this system (Marchenko et al 2000). As a result of the large number of orbits which have elapsed, the listed phases are only approximate and do not account for the apsidal motion detected in Iota Orionis (Stickland et al 1987;Marchenko et al 2000).…”

Section: P R E V I O U S X -R Ay O B S E Rvat I O N S O F I O Ta O R mentioning

confidence: 99%

“…In column 3 we list the orbital phase at the time of observation, calculated from the ephemeris HJD periastron 2451 121X658 1 29X133 76E derived from the latest optical monitoring of this system (Marchenko et al 2000). As a result of the large number of orbits which have elapsed, the listed phases are only approximate and do not account for the apsidal motion detected in Iota Orionis (Stickland et al 1987;Marchenko et al 2000). We also draw attention to the different count rates obtained by different authors when analysing the same data sets, and the relatively constant count rates obtained from different data sets by the same authors.…”

Section: P R E V I O U S X -R Ay O B S E Rvat I O N S O F I O Ta O R mentioning

confidence: 99%

“…The new ASCA observations were coordinated with an extensive set of ground-based optical observations reported in Marchenko et al (2000). In this work, the spectra of the components were successfully separated, allowing the refinement of the orbital elements (including the restriction of the orbital inclination to 508 & i & 708 and confirmation of the rapid apsidal motion.…”

mentioning

confidence: 99%

See 2 more Smart Citations

Coordinated monitoring of the eccentric O-star binary Iota Orionis: the X-ray analysis

Pittard

Stevens

Corcoran

et al. 2002

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

We analyse two ASCA observations of the highly eccentric O9 III+B1 III binary Iota Orionis obtained at periastron and apastron. Based on the assumption of a strong colliding‐wind shock between the stellar components, we expected to see significant variation in the X‐ray emission between these phases. The observations proved otherwise: the X‐ray luminosities and spectral distributions were remarkably similar. The only noteworthy feature in the X‐ray data was the hint of a proximity effect during periastron passage. Although this ‘flare’ is of relatively low significance, it is supported by the notable proximity effects seen in the optical, and the phasing of the X‐ray and optical events is in very good agreement. However, other interpretations are also possible. In view of the degradation of the SIS instrument and source contamination in the GIS data we discuss the accuracy of these results, and also analyse archival ROSAT observations. We investigate why we do not see a clear colliding‐wind signature. A simple model shows that the wind attenuation to the expected position of the shock apex is negligible throughout the orbit, which poses the puzzling question of why the expected 1/D variation (i.e. a factor of 7.5) in the intrinsic luminosity is not seen in the data. Two scenarios are proposed: either the colliding‐wind emission is unexpectedly weak such that intrinsic shocks in the winds dominate the emission, or, alternatively, the emission observed is colliding‐wind emission but in a more complex form than we would naively expect. Complex hydrodynamical models are then analysed. Despite strongly phase‐variable emission from the models, both are consistent with the observations. We find that if the mass‐loss rates of the stars are low then intrinsic wind shocks could dominate the emission. However, when we assume higher mass‐loss rates of the stars, we find that the observed emission could also be consistent with a purely colliding‐wind origin. A summary of the strengths and weaknesses of each interpretation is presented. To distinguish between the different models X‐ray observations with improved phase coverage will be necessary.

show abstract

Radial velocity measurements of the runaway stars AE Aur and ι Ori

Heyne¹,

Mugrauer²,

Bischoff³

et al. 2020

Astron Nachr

View full text Add to dashboard Cite

We present the results of our spectroscopic monitoring observations of the late O‐type runaway stars AE Aur and ι Ori, carried out between September 2016 and May 2018 using the Échelle spectrograph FLECHAS at the University Observatory Jena. For both stars, we obtained current radial velocity (RV) measurements with better precision than before. These results can be used for further advanced calculations of their space motion, needed to determine, for example, their place of origin in our Galaxy. In this paper, we describe the observations and the data reduction, as well as the analysis of all spectral data. We find a stable RV for AE Aur and confirm ι Ori as a double‐lined spectroscopic binary and derive its current Keplerian orbital elements.

show abstract

Coordinated monitoring of the eccentric O-star binary Iota Orionis: optical spectroscopy and photometry

Cited by 19 publications

References 37 publications

Phase-resolved X-ray and optical spectroscopy of the massive binary HD 93403

Phase-resolved X-ray and optical spectroscopy of the massive binary HD 93403

Coordinated monitoring of the eccentric O-star binary Iota Orionis: the X-ray analysis

Radial velocity measurements of the runaway stars AE Aur and ι Ori

Contact Info

Product

Resources

About